Abstract Details
| Name: Manoj Puravankara Affiliation: Tata Institute of Fundamental Research Conference ID: ASI2015_522 Title : Herschel spectral mapping of the OMC-2 region: spatial distribution and excitation conditions of the shocked gas in outflows from protostars Authors and Co-Authors : B. Gonzalez_Garcia, R. Vavrek (HSC, ESA, Madrid, Spain), D. Watson (Univ. of Rochester, USA), S. T. Megeath (Univ. Of Toledo, USA) & the Herschel Orion Protostar Survey (HOPS) team Abstract Type : Poster Abstract Category : Stars, The Milky Way Galaxy and its neighbours Abstract : The OMC-2 region is one of the most active star-forming complex in the Orion A cloud and contains some of the most luminous protostars in the entire Orion cloud, notably OMC-2 FIR 3 and FIR 4. These protostars are also the brightest line emitters among the low-mass protostars observed with Herschel. The low excitation CO observations show collimated outflows centered on the more luminous FIR 3, with one lobe extending up to FIR 4; no evidence for outflow from FIR 4 is seen in the low excitation line maps. We have obtained and analysed high spatial resolution spectral line maps of the OMC-2 region centered around these two protostars with the PACS and SPIRE instrument onboard Herschel. Spatial distribution of molecular lines (CO, H2O & OH) and fine structure lines ([OI] & [CII]) observed with Herschel indicate that currently shocked gas (T = several 100s to a few 1000 K) traced by the high-excitation lines in the far-infrared have a very different morphology and spatial distribution than the cold gas (T < 100 K) traced by low excitation submm/mm molecular lines. High excitation line maps appear to indicate the presence of a powerful, but compact outflow driven by FIR 4. We have further analysed the excitation conditions of the hot and warm emitting gas surrounding these two protostars to study the mechanisms responsible for the heating of the gas in the OMC-2 region. We will present our analysis and results in this contribution. |